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<ri:Resource created="2021-09-24T06:54:41Z" status="active" updated="2025-05-19T09:50:00Z" version="1.2" xmlns:cs="http://www.ivoa.net/xml/ConeSearch/v1.0" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/ConeSearch/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/ConeSearch.xsd http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>THYME. V. Discovering a new stellar association</title><shortName>J/AJ/161/171</shortName><identifier>ivo://CDS.VizieR/J/AJ/161/171</identifier><altIdentifier>doi:10.26093/cds/vizier.51610171</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Tofflemire B.M.</name></creator><creator><name>Rizzuto A.C.</name></creator><creator><name>Newton E.R.</name></creator><creator><name>Kraus A.L.</name></creator><creator><name>Mann A.W.,Vanderburg A.</name></creator><creator><name>Nelson T.</name></creator><creator><name>Hawkins K.</name></creator><creator><name>Wood M.L.</name></creator><creator><name>Zhou G.</name></creator><creator><name>Quinn S.N.,Howell S.B.</name></creator><creator><name>Collins K.A.</name></creator><creator><name>Schwarz R.P.</name></creator><creator><name>Stassun K.G.</name></creator><creator><name>Bouma L.G.,Essack Z.</name></creator><creator><name>Osborn H.</name></creator><creator><name>Boyd P.T.</name></creator><creator><name>Furesz G.</name></creator><creator><name>Glidden A.</name></creator><creator><name>Twicken J.D.,Wohler B.</name></creator><creator><name>McLean B.</name></creator><creator><name>Ricker G.R.</name></creator><creator><name>Vanderspek R.</name></creator><creator><name>Latham D.W.</name></creator><creator><name>Seager S.,Winn J.N.</name></creator><creator><name>Jenkins J.M.</name></creator><date role="Updated">2024-10-11T20:10:03Z</date><date role="Created">2021-09-24T06:54:41Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><subject>stellar-associations</subject><subject>infrared-photometry</subject><subject>visible-astronomy</subject><subject>radial-velocity</subject><description>The detection and characterization of young planetary systems offer a direct path to study the processes that shape planet evolution. We report on the discovery of a sub-Neptune-sized planet orbiting the young star HD110082 (TOI-1098). Transit events we initially detected during TESS Cycle 1 are validated with time-series photometry from Spitzer. High-contrast imaging and high-resolution, optical spectra are also obtained to characterize the stellar host and confirm the planetary nature of the transits. The host star is a late-F dwarf (M*=1.2M{sun}) with a low-mass, M dwarf binary companion (M*=0.26M{sun}) separated by nearly one arcminute (~6200au). Based on its rapid rotation and Lithium absorption, HD110082 is young, but is not a member of any known group of young stars (despite proximity to the Octans association). To measure the age of the system, we search for coeval, phase-space neighbors and compile a sample of candidate siblings to compare with the empirical sequences of young clusters and to apply quantitative age-dating techniques. In doing so, we find that HD110082 resides in a new young stellar association we designate MELANGE-1, with an age of 250_-70_^+50^Myr. Jointly modeling the TESS and Spitzer light curves, we measure a planetary orbital period of 10.1827days and radius of Rp=3.2{+/-}0.1R{Earth}. HD110082b's radius falls in the largest 12% of field-age systems with similar host-star mass and orbital period. This finding supports previous studies indicating that young planets have larger radii than their field-age counterparts.</description><source format="bibcode">2021AJ....161..171T</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/161/171</referenceURL><type>Catalog</type><contentLevel>Research</contentLevel><relationship><relationshipType>IsServedBy</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/TAP">TAP VizieR generic service</relatedResource></relationship><relationship><relationshipType>IsServedBy</relationshipType><relatedResource>Conesearch service</relatedResource></relationship><relationship><relationshipType>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/I/259">I/259 : The Tycho-2 Catalogue (Hog+ 2000)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/305">I/305 : The Guide Star Catalog, Version 2.3.2 (GSC2.3) (STScI, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/337">I/337 : Gaia DR1 (Gaia Collaboration, 2016)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/II/335">II/335 : Revised catalog of GALEX UV sources (GUVcat_AIS GR6+7)(Bianchi+ 2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/347">I/347 : Distances to 1.33 billion stars in Gaia DR2 (Bailer-Jones+, 2018)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/345">I/345 : Gaia DR2 (Gaia Collaboration, 2018)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/II/358">II/358 : SkyMapper Southern Sky Survey. 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